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arxiv: 2607.00105 · v1 · pith:5MBSOOJJnew · submitted 2026-06-30 · 🌌 astro-ph.GA · astro-ph.HE

AGN radiative feedback as the main regulator of [O III] outflow activity and obscuration in X-ray AGN

Carolina Andonie , Andrea Merloni , Catarina Aydar , Benny Trakhtenbrot , Johannes Buchner , Brivael Laloux , Mara Salvato , Peter Boorman
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David M. Alexander Marcella Brusa Pietro Baldini Tiago Costa Victoria A. Fawcett Zsofi Igo Kirpal Nandra
This is my paper

Pith reviewed 2026-07-02 18:07 UTC · model grok-4.3

classification 🌌 astro-ph.GA astro-ph.HE
keywords AGNEddington ratioionized outflowsX-ray obscurationradiative feedback[O III]eROSITA
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The pith

Eddington ratio drives ionized outflow incidence and X-ray obscuration levels in AGN once luminosity is matched.

A machine-rendered reading of the paper's core claim, the machinery that carries it, and where it could break.

The paper shows that the fraction of AGN with powerful [O III] outflows rises from 29 percent at low Eddington ratios to 50 percent at high ones, while X-ray obscuration drops by a factor of five over the same range. These trends disappear when AGN samples are matched on luminosity, which isolates the Eddington ratio as the controlling variable rather than black hole mass. The result supports radiative feedback models in which radiation pressure from high-accretion-rate AGN clears circumnuclear material and launches galaxy-scale outflows. A reader would care because it supplies direct evidence that accretion rate, not mass, sets the observable feedback signatures in a large, uniform X-ray-selected sample.

Core claim

Radiation pressure tied to the Eddington ratio regulates both the incidence of [O III] outflows and the amount of X-ray obscuration, while black hole mass plays no significant independent role. This is shown by the disappearance of all trends with Eddington ratio once samples are matched on AGN luminosity, leaving only the short-lived high-outflow phase in the forbidden region of the NH–lambda plane.

What carries the argument

Luminosity-matched comparison of Eddington-ratio subsamples to isolate radiation-pressure effects from black-hole-mass effects.

Load-bearing premise

Matching samples solely on AGN luminosity removes all influence of black hole mass and leaves only radiation pressure as the cause of remaining differences.

What would settle it

Repeating the analysis after direct black-hole-mass measurements and matching on both luminosity and black-hole mass, then finding that outflow incidence or obscuration still correlates with Eddington ratio, would support the claim; persistent correlation with mass instead would falsify it.

Figures

Figures reproduced from arXiv: 2607.00105 by Andrea Merloni, Benny Trakhtenbrot, Brivael Laloux, Carolina Andonie, Catarina Aydar, David M. Alexander, Johannes Buchner, Kirpal Nandra, Mara Salvato, Marcella Brusa, Peter Boorman, Pietro Baldini, Tiago Costa, Victoria A. Fawcett, Zsofi Igo.

Figure 1
Figure 1. Figure 1: Stacked [O iii] velocity profile of the sources in our sample with log LAGN/(erg s−1 ) = 45 − 45.5. The profile is normalised to the [O iii] peak flux and shows a clear asymmetry. The figure also shows the velocity at which the integrated line flux reaches 5%, 10%, 90%, and 95% of the total, which are used to calculate the kinematic param￾eters W80 and ∆v. Fe II continuum estimated with PyQSOFit, and also … view at source ↗
Figure 2
Figure 2. Figure 2: Non-parametric [O iii] velocity (W80) plotted against intrinsic soft X-ray luminosity (L0.5−2 keV; bottom x-axis) and AGN bolometric luminosity (LAGN, derived from L0.5−2 keV; top x-axis). Only sources with a significant [O iii] detection are shown. The y-axis error bars represent the 1σ uncertainties in W80; the mean x-axis error is indicated by a green marker with error bars in the upper left side of the… view at source ↗
Figure 4
Figure 4. Figure 4: Top: Non-parametric [O iii] velocity W80 against the logarithmic Eddington ratio log λEdd. The plot shows three samples with different Eddington ratios: log λEdd < −2.3 (cyan circles), −2.3 < log λEdd < −1.7 (green stars), and log λEdd > −1.7 (orange squares). The horizon￾tal dotted line at W80 = 600 km s−1 shows the threshold typically used to identify outflows. The top panel of the figure displays the ou… view at source ↗
Figure 10
Figure 10. Figure 10: We first fit the rest-frame 2-5 keV stacks using an ab [PITH_FULL_IMAGE:figures/full_fig_p009_10.png] view at source ↗
Figure 6
Figure 6. Figure 6: Top panels: Distributions of the non-parametric velocity (W80) and asymmetry (∆v) of the same sample λEdd MBH − z matched samples plotted in [PITH_FULL_IMAGE:figures/full_fig_p010_6.png] view at source ↗
Figure 5
Figure 5. Figure 5: Same as [PITH_FULL_IMAGE:figures/full_fig_p010_5.png] view at source ↗
Figure 7
Figure 7. Figure 7: Stacked [O iii] spectra for the same Eddington ratio matched samples as in [PITH_FULL_IMAGE:figures/full_fig_p010_7.png] view at source ↗
Figure 8
Figure 8. Figure 8: Line of sight column density NH against Eddington ratio log λEdd. The plot shows three samples with different Eddington ratios: log λEdd < −2.3 (cyan circles), −2.3 < log λEdd < −1.7 (green stars), and log λEdd > −1.7 (orange squares). The top panel of the figure displays the fraction of sources with log NH/cm−2 > 21, fobs, 21, in each Eddington ratio sam￾ple. The error bars correspond to 1σ uncertainties … view at source ↗
Figure 9
Figure 9. Figure 9: Top panels: distributions (left) and cumulative distributions (right) of the line of sight column densities NH of sources with log λEdd < −2.3 (cyan dotted), −2.3 < log λEdd < −1.7 (green dashed), and log λEdd > −1.7 (orange solid). The vertical lines indicate the mean NH of each λEdd sample. Bottom panels: same as the top panels, but the Eddington ratio samples are matched in MBH and redshift. As in the p… view at source ↗
Figure 11
Figure 11. Figure 11: Left panel: Line of sight column density, NH, against the Eddington ratio, log λEdd for our sample with broad Hβ detections. The black curve corresponds to the effective Eddington ratio (λ Eff Edd) for the dust composition of the Milky Way ISM, taken from Fabian et al. (2009). The NH −λEdd plane is subdivided into 6 different sections, and for each one, we calculate the outflow occurrence rate, fout. The … view at source ↗
read the original abstract

Large-scale ionised outflows and nuclear obscuration are fundamental manifestations of AGN activity, yet direct observational evidence linking these phenomena remains scarce. We use the eROSITA Final Equatorial Depth Survey, among the largest uniform optical spectroscopic datasets of X-ray AGN, to investigate how AGN accretion rate affects ionised outflow kinematics and X-ray obscuration. Our sample comprises 2.840 AGN at z<0.82 with high-quality SDSS spectra. Through optical spectral fitting, we measure Eddington ratios ($\lambda_{Edd}$) and [O III] emission-line kinematics, tracing ionised outflows. In addition, we use archival eROSITA X-ray spectroscopy with X-ray stacking analyses to constrain the obscuration of the sample, $N_H$. We find that (1) 35% of the entire sample hosts a [O III] outflows ($W_{80}>600$ km/s), with the outflow incidence increasing with the AGN luminosity from 15% at $L_{AGN}<10^{44}$ erg/s up to 60% at $L_{AGN}>10^{46}$ erg/s; (2) the outflow incidence increases with Eddington ratio from 29% at $\log \lambda_{Edd}<-2.3$ to 50% at $\log \lambda_{Edd}>-1.7$; and (3) the AGN obscuration decreases with Eddington ratio, as sources with $\log\lambda_{Edd}>-1.7$ are 5 times less obscured than lower Eddington ratios AGN. In addition, we find that 1% of the sample populates the "forbidden region" of the $N_H-\lambda_{Edd}$ plane, where the outflow incidence peaks at 52%, consistent with a short-lived feedback phase. Notably, when matching the Eddington ratios samples in AGN luminosity, these trends vanish, implying that radiation pressure drives changes in outflow activity and obscuration, while the black hole mass does not play a significant role. Our results are in agreement with AGN radiative feedback scenarios, where the Eddington ratio regulates the AGN environment by driving powerful, galaxy-wide outflows and shaping the amount of circumnuclear material.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit. Tearing a paper down is the easy half of reading it; the pith above is the substance, this is the friction.

Referee Report

1 major / 2 minor

Summary. The manuscript analyzes 2840 X-ray AGN at z<0.82 from the eROSITA Final Equatorial Depth Survey with SDSS spectra. It measures Eddington ratios and [O III] kinematics (W_80>600 km/s for outflows) via optical spectral fitting and constrains obscuration N_H via eROSITA X-ray spectroscopy and stacking. Key findings: outflow incidence rises from 15% at L_AGN<10^44 erg/s to 60% at L_AGN>10^46 erg/s and from 29% at log λ_Edd<-2.3 to 50% at log λ_Edd>-1.7; obscuration drops by a factor of 5 at high λ_Edd; 1% of sources occupy a 'forbidden region' in the N_H-λ_Edd plane with 52% outflow incidence. After matching Eddington-ratio subsamples on AGN luminosity, trends vanish, implying radiation pressure via λ_Edd (not black hole mass) regulates outflows and obscuration, consistent with radiative feedback models.

Significance. If the luminosity-matching test holds after addressing the noted degeneracy, the result would strengthen observational evidence for radiative feedback in which Eddington ratio drives galaxy-scale outflows and modulates circumnuclear obscuration. The large, uniform X-ray-selected sample with high-quality spectroscopy and the combination of kinematic and X-ray stacking analyses constitute clear strengths; the identification of the forbidden region with elevated outflow activity is a potentially falsifiable prediction worth highlighting.

major comments (1)
  1. [Abstract] Abstract (final paragraph on luminosity matching): the claim that matching Eddington-ratio subsamples on AGN luminosity implies 'radiation pressure drives changes in outflow activity and obscuration, while the black hole mass does not play a significant role' is not supported by the described test. Because λ_Edd ≡ L_AGN / L_Edd and L_Edd ∝ M_BH, any two subsamples at identical L_AGN but differing λ_Edd necessarily differ in M_BH by the inverse factor; the procedure therefore leaves λ_Edd and M_BH perfectly degenerate. The vanishing of trends is equally consistent with no residual dependence on either quantity once L_AGN is controlled, so the inference that M_BH plays no role does not logically follow.
minor comments (2)
  1. The definition of the 'forbidden region' in the N_H-λ_Edd plane and the exact binning or selection criteria yielding the 52% outflow incidence should be stated explicitly (currently only noted in the abstract).
  2. Methods section on spectral fitting: the precise definition of W_80, the velocity threshold choice, and how uncertainties from line-profile decomposition propagate into the reported incidence percentages (15%, 29%, 50%, etc.) are not detailed in the abstract and would benefit from a dedicated methods subsection or table.

Simulated Author's Rebuttal

1 responses · 0 unresolved

We thank the referee for their careful reading and constructive feedback on our manuscript. We address the single major comment below.

read point-by-point responses

  1. Referee: [Abstract] Abstract (final paragraph on luminosity matching): the claim that matching Eddington-ratio subsamples on AGN luminosity implies 'radiation pressure drives changes in outflow activity and obscuration, while the black hole mass does not play a significant role' is not supported by the described test. Because λ_Edd ≡ L_AGN / L_Edd and L_Edd ∝ M_BH, any two subsamples at identical L_AGN but differing λ_Edd necessarily differ in M_BH by the inverse factor; the procedure therefore leaves λ_Edd and M_BH perfectly degenerate. The vanishing of trends is equally consistent with no residual dependence on either quantity once L_AGN is controlled, so the inference that M_BH plays no role does not logically follow.

    Authors: We agree with the referee that the luminosity-matching procedure leaves λ_Edd and M_BH degenerate, since subsamples at fixed L_AGN but different λ_Edd must differ in M_BH by the inverse factor. The vanishing of trends after matching therefore shows that the observed dependencies are not independent of L_AGN, but does not permit the stronger claim that M_BH plays no role. We will revise the abstract and the relevant discussion sections to remove the statement that black hole mass does not play a significant role. The revised text will state that the results remain consistent with radiative feedback regulated by Eddington ratio, while explicitly noting the degeneracy with black hole mass at fixed luminosity. This change will be incorporated in the resubmitted version. revision: yes

Circularity Check

0 steps flagged

Observational correlation study with no circular derivation chain

full rationale

The paper reports empirical trends from eROSITA/SDSS data using standard spectral fitting to measure λ_Edd, [O III] kinematics, and N_H, followed by a luminosity-matching control. No equations, derivations, or first-principles results are presented that reduce to fitted parameters by construction. No self-citation load-bearing steps, uniqueness theorems, or ansatzes are invoked. The central claim rests on observational controls and data, remaining self-contained against external benchmarks.

Axiom & Free-Parameter Ledger

2 free parameters · 2 axioms · 0 invented entities

Observational study resting on standard domain assumptions about emission-line diagnostics and X-ray absorption; thresholds for binning and outflow definition are study-specific choices.

free parameters (2)
  • Outflow velocity threshold = 600 km/s
    W80 > 600 km/s used to classify outflows
  • Eddington ratio bin edges = -2.3 and -1.7
    log λ_Edd = -2.3 and -1.7 used to separate regimes
axioms (2)
  • domain assumption [O III] line width traces ionized outflows
    Standard assumption invoked when measuring outflow incidence from optical spectra
  • domain assumption X-ray spectral fitting and stacking constrain line-of-sight N_H
    Standard method for measuring obscuration in the abstract

pith-pipeline@v0.9.1-grok · 6010 in / 1411 out tokens · 50890 ms · 2026-07-02T18:07:00.143826+00:00 · methodology

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